Table C.1.
Photometric upper limits in multiple bands computed from our X-shooter spectra.
| Object | B | V | G | R | I | Y | J | H | Ks |
|---|---|---|---|---|---|---|---|---|---|
| S1 | 21.3 ± 0.4 | 20.8 ± 0.4 | 19.9 ± 0.3 | 19.7 ± 0.4 | 18.7 ± 0.5 | 18.6 ± 0.3 | 17.9 ± 0.2 | 16.8 ± 0.4 | 16.1 ± 0.3 |
| S1-SE | 22.5 ± 0.7 | 21.4 ± 0.4 | 20.3 ± 0.3 | 20.1 ± 0.4 | 18.9 ± 0.5 | 18.6 ± 0.2 | 17.8 ± 0.2 | 16.6 ± 0.5 | 15.7 ± 0.3 |
| S2 | – | – | – | – | – | – | 21.6 ± 3.4 | 17.9 ± 3.3 | 15.7 ± 0.4 |
| S3 | – | – | 19.7 ± 0.5 | 19.0 ± 0.5 | 18.7 ± 0.6 | 18.9 ± 0.4 | 18.6 ± 0.4 | 17.4 ± 0.5 | 15.8 ± 0.5 |
| S3-K | 20.4 ± 0.4 | 19.0 ± 0.3 | 17.4 ± 0.3 | 17.3 ± 0.3 | 15.7 ± 0.4 | 15.3 ± 0.3 | 15.0 ± 0.2 | 13.7 ± 0.3 | 13.2 ± 0.3 |
| S4 | 19.1 ± 0.4 | 19.0 ± 0.4 | 18.2 ± 0.3 | 18.0 ± 0.4 | 17.1 ± 0.5 | 17.3 ± 0.3 | 16.7 ± 0.2 | 14.5 ± 0.3 | 12.7 ± 0.3 |
| S5-A | 16.8 ± 0.4 | 16.6 ± 0.4 | 16.2 ± 0.4 | 15.9 ± 0.4 | 15.5 ± 0.4 | 16.1 ± 0.3 | 16.9 ± 0.2 | 16.4 ± 0.4 | 16.2 ± 0.3 |
| S5-B | 19.1 ± 0.5 | 19.1 ± 0.4 | 18.7 ± 0.4 | 18.5 ± 0.5 | 18.2 ± 0.4 | 19.0 ± 0.3 | 19.9 ± 0.6 | 19.6 ± 2.4 | 18.9 ± 3.1 |
| S5-C | 18.3 ± 0.4 | 18.4 ± 0.4 | 18.2 ± 0.6 | 18.4 ± 0.5 | 18.1 ± 0.4 | 19.0 ± 0.3 | 20.1 ± 0.6 | 19.7 ± 3.1 | 20.5 ± 5.1 |
| S5-D | 20.6 ± 0.6 | 20.0 ± 0.4 | 19.1 ± 0.3 | 18.7 ± 0.4 | 17.9 ± 0.4 | 18.3 ± 0.3 | 18.3 ± 0.3 | 17.2 ± 3.9 | 17.3 ± 0.5 |
| S5-E | 20.6 ± 0.6 | 19.8 ± 0.5 | 19.5 ± 0.6 | 19.0 ± 0.6 | 19.3 ± 0.4 | 19.4 ± 0.3 | 20.0 ± 0.5 | 18.0 ± 0.4 | 15.0 ± 0.3 |
| S5-F | 17.8 ± 0.4 | 17.6 ± 0.5 | 17.5 ± 0.6 | 17.7 ± 0.4 | 17.2 ± 0.6 | 18.1 ± 0.4 | 19.4 ± 0.5 | 18.9 ± 2.5 | 17.4 ± 0.8 |
| S6 | – | 17.9 ± 0.7 | 18.1 ± 1.1 | – | 20.2 ± 1.0 | 18.4 ± 0.4 | 17.2 ± 0.2 | 14.8 ± 0.5 | 13.2 ± 0.3 |
| S7-A | 17.9 ± 0.4 | 17.8 ± 0.4 | 17.5 ± 0.4 | 17.4 ± 0.5 | 17.2 ± 0.5 | 17.5 ± 0.3 | 16.6 ± 0.2 | 14.8 ± 0.3 | 13.2 ± 0.3 |
| S7-B | 19.7 ± 0.4 | 19.2 ± 0.4 | 18.7 ± 0.3 | 18.4 ± 0.4 | 17.8 ± 0.6 | 18.6 ± 0.6 | 17.7 ± 0.2 | 15.3 ± 0.3 | 13.1 ± 0.3 |
| S8 | 21.9 ± 0.5 | 20.8 ± 0.4 | 19.5 ± 0.3 | 19.4 ± 0.4 | 18.0 ± 0.5 | 17.8 ± 0.3 | 17.6 ± 0.3 | 16.2 ± 0.5 | 14.9 ± 0.4 |
| S9 | – | 21.1 ± 0.5 | 20.9 ± 0.5 | 20.8 ± 0.5 | 20.0 ± 0.6 | 20.1 ± 0.6 | 19.8 ± 0.8 | 17.4 ± 2.3 | 15.6 ± 3.7 |
| S10-A | – | 21.1 ± 0.5 | 20.9 ± 0.5 | 21.0 ± 0.6 | 20.0 ± 0.7 | 20.9 ± 1.3 | 20.8 ± 1.8 | – | 16.2 ± 0.5 |
| S10-BC | – | 21.0 ± 0.5 | 20.8 ± 0.5 | 20.6 ± 0.6 | 20.0 ± 0.6 | 20.4 ± 0.7 | 20.0 ± 0.7 | 18.0 ± 0.6 | 16.4 ± 0.4 |
| S10-K | – | 21.1 ± 0.6 | 21.1 ± 0.7 | 21.2 ± 1.2 | 20.5 ± 0.7 | 21.5 ± 2.9 | 20.2 ± 0.8 | 17.5 ± 2.8 | 15.8 ± 0.4 |
| S10-SW-A | 22.4 ± 0.7 | 21.2 ± 0.4 | 20.1 ± 0.4 | 19.7 ± 0.4 | 18.8 ± 0.6 | 18.6 ± 0.3 | 17.7 ± 0.2 | 16.1 ± 0.5 | 14.7 ± 0.3 |
| S10-SW-B | – | 22.3 ± 0.8 | 22.4 ± 1.2 | 22.8 ± 2.4 | 23.3 ± 6.7 | 21.0 ± 1.3 | 19.7 ± 0.4 | 17.9 ± 0.4 | 16.6 ± 0.4 |
| R135 | 13.5 ± 0.5 | 13.7 ± 0.4 | 13.2 ± 0.5 | 12.9 ± 0.5 | 12.9 ± 0.4 | 13.4 ± 0.2 | 13.4 ± 0.2 | 13.2 ± 0.3 | 13.1 ± 0.3 |
Notes. All magnitudes are upper limits computed using Eq. (1). For the B, V, R, and I-bands we used the Bessell photometric system (Bessell 1990), for the G-band we used the Gaia photometric system (Gaia Collaboration 2016), and for the Y, J, H and Ks-bands we used the VISTA photometric system. The empty band values resulted from a negative integrated flux in the corresponding band. The objects shown in bold are the MYSOs confirmed in this work.
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